Gamma-rays from radioactive 26Al (half-life 7.2 × 105 years) provide a ‘snapshot’ view of continuing nucleosynthesis in the Galaxy1. The Galaxy is relatively transparent to such γ-rays, and emission has been found concentrated along its plane2. This led to the conclusion1 that massive stars throughout the Galaxy dominate the production of 26Al. On the other hand, meteoritic data show evidence for locally produced 26Al, perhaps from spallation reactions in the protosolar disk3,4,5. Furthermore, prominent γ-ray emission from the Cygnus region suggests that a substantial fraction of Galactic 26Al could originate in localized star-forming regions. Here we report high spectral resolution measurements of 26Al emission at 1808.65 keV, which demonstrate that the 26Al source regions corotate with the Galaxy, supporting its Galaxy-wide origin. We determine a present-day equilibrium mass of 2.8 (± 0.8) solar masses of 26Al. We use this to determine that the frequency of core collapse (that is, type Ib/c and type II) supernovae is 1.9 (± 1.1) events per century.

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  1. 1.

    & Radioactive 26Al in the Galaxy: observations versus theory. Phys. Rep. 267(1), 1– 69 (1996)

  2. 2.

    et al. COMPTEL observations of Galactic 26Al. Astron. Astrophys. 298, 445– 460 (1995)

  3. 3.

    , & Distribution of 26Al in the early solar system. Meteoritics 30, 365– 386 (1995)

  4. 4.

    et al. Supra-canonical 26Al/27Al and the residence time of CAIs in the solar protoplanetary disk. Science 308, 223– 227 (2005)

  5. 5.

    et al. Protostellar cosmic rays and extinct radioactivities in meteorites. Astrophys. J. 506, 898– 912 (1998)

  6. 6.

    Isolated star formation: from cloud formation to core collapse. Science 295, 76– 81 (2002)

  7. 7.

    & Short-lived radioactivities and the birth of the Sun. Space Sci. Rev. 92, 133– 152 (2000)

  8. 8.

    , et al. in Exploring the Gamma-Ray Universe (4th INTEGRAL Workshop) (eds Gimenez, A., Reglero, V. & Winkler, C.) 55– 58 (ESA Special Publication, ESA-SP 459, Noordwijk, 2001)

  9. 9.

    , & Line shape diagnostics of Galactic 26Al. Astron. Astrophys. 412, L77– L81 (2003)

  10. 10.

    et al. A multiwavelength comparison of COMPTEL 26Al line data. Astron. Astrophys. 344, 68– 82 (1999)

  11. 11.

    & Pulsar distances and the Galactic distribution of free electrons. Astrophys. J. 411, 674– 684 (1993)

  12. 12.

    Cordes, J. M. & Lazio, T. J. W. NE2001. I. A new model for the Galactic distribution of free electrons and its variability. Preprint at (2002).

  13. 13.

    , , & A synthetic view on structure and evolution of the Milky Way. Astron. Astrophys. 409, 523– 540 (2003)

  14. 14.

    Asplund, M, Grevesse, N. & Sauval, A. J. in Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis in Honor of David L. Lambert Vol. 336 25–39 (ASP Conf. Ser., 2005).

  15. 15.

    The star formation history of the Milky Way. ASP Conf. Proc. 230, 3– 12 (2001)

  16. 16.

    & Chemo-spectrophotometric evolution of spiral galaxies—I. The model and the Milky Way. Mon. Not. R. Astron. Soc. 307, 857– 876 (1999)

  17. 17.

    & The luminosity function of OB associations in the Galaxy. Astrophys. J. 476, 144– 165 (1997)

  18. 18.

    New estimates of the solar-neighborhood massive star birthrate and the Galactic supernova rate. Astron. J. 130, 1652– 1657 (2005)

  19. 19.

    , , & Nucleosynthesis in massive stars with improved nuclear and stellar physics. Astrophys. J. 576, 323– 348 (2002)

  20. 20.

    & 26Al and 60Fe from massive stars. Nucl. Phys. A 758, 11c– 14c (2005)

  21. 21.

    et al. New estimates of the contribution of Wolf Rayet stellar winds to the Galactic 26Al. Astron. Astrophys. 429, 613– 624 (2005)

  22. 22.

    The initial mass function of stars. Science 295, 82– 91 (2002)

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This paper is based on observations with INTEGRAL, an ESA project with instruments and a science data center funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), Czech Republic and Poland, and with the participation of Russia and the USA. The SPI project has been completed under the responsibility and leadership of CNES/France. The SPI anticoincidence system is supported by the German government. We are grateful to ASI, CEA, CNES, DLR, ESA, INTA, NASA and OSTC for support. We are grateful to Alessandro Chieffi, Nikos Prantzos, and Stan Woosley for discussions of theoretical nucleosynthesis yields.

Author information


  1. Max-Planck-Institut für extraterrestrische Physik, D-85748 Garching, Germany

    • Roland Diehl
    • , Hubert Halloin
    • , Karsten Kretschmer
    • , Giselher G. Lichti
    • , Volker Schönfelder
    • , Andrew W. Strong
    • , Andreas von Kienlin
    •  & Wei Wang
  2. Centre d'Etude Spatiale des Rayonnements and Université Paul Sabatier, 31028 Toulouse, France

    • Pierre Jean
    • , Jürgen Knödlseder
    • , Jean-Pierre Roques
    •  & Georg Weidenspointner
  3. DSM/DAPNIA/Service d'Astrophysique, CEA Saclay, 91191 Gif-Sur-Yvette, France

    • Stephane Schanne
  4. Clemson University, Clemson, South Carolina 29634-0978, USA

    • Dieter H. Hartmann
  5. ESA/ESTEC, SCI-SD 2201 AZ Noordwijk, The Netherlands

    • Christoph Winkler
  6. Space Sciences Laboratory, Berkeley, California 94720, USA

    • Cornelia Wunderer


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Correspondence to Roland Diehl.

Supplementary information

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  1. 1.

    Supplementary Methods

    Observations and Data. The INTEGRAL Observatory and its spectrometer instrument have been launched in Oct 2002. Observations are composed of 7130 pointings along the plane of the Galaxy, and sum up to an exposure of 4 Ms at the Galactic Center, from the first two years of the mission.

  2. 2.

    Supplementary Methods

    Data Analysis and Results. Spectra are determined from independent model fits in 0.5 keV bins. Splitting the sky model into longitude segments allows for spatially-resolved spectroscopy, and obtains Doppler shifts as expected from Galactic rotation. The variability of resulting spectra with different models for the spatial distribution of 26Al emission is modest to small.

  3. 3.

    Supplementary Discussion

    Doppler Broadening. The width of the observed gamma-ray line depends on the state of the ISM.

  4. 4.

    Supplementary Discussion

    Galactic Rotation. Different models for the spatial distribution of 26Al emission and rotation curves for the inner Galaxy lead to variations in expected line shifts.

  5. 5.

    Supplementary Discussion

    Nucleosynthesis Yields. Different models for stellar evolution and supernovae predict somewhat different yields of 26Al. From current models, an assessment is made over the full range of massive stars.

  6. 6.

    Supplementary Methods

    Deriving a Galactic Star Formation Rate from 26Al Gamma-rays. The determination of the supernova rate follows from the nucleosynthesis yield and its integration over the mass distribution of stars. The conversion to a star formation rate is described.

  7. 7.

    Supplementary Discussion

    Star Formation Rate (SFR) and Supernova Rate (SNR) Estimates for the Galaxy. The different approaches determining supernova rates or star formation rates for the Galaxy are presented in a Table, with discussion of strengths and weaknesses. The 26Al-based approach is completely independent, and among the less-biased and more accurate methods.

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